Solar Internal Stresses: Rotation and Magnetic Fields

Ulrich, Roger K.

doi:10.1007/978-94-009-5253-9_6

Roger K. Ulrich⁵

Part of the book series: Geophysics and Astrophysics Monographs ((GAAM,volume 24))

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Abstract

The theory of rotating, self-gravitating objects is very old, going back to much names as Newton, Clairaut, and Maclaurin in the seventeenth and eighteenth centuries. Important applications to stars were made in the 1920s by von Zeipel (1924a, b), Eddington (1925, 1926, 1929), and Vogt (1925). Although the problems of rotating stars can be stated relatively easily, realistic solutions are enormously difficult to obtain. The study of the subject of rotating stars has been greatly aided by the recent publication of an excellent monograph by Tassoul (1978) which gives a very complete review of the field and makes an extensive introduction to this chapter unnecessary. Tassoul’s book has been heavily drawn upon in the preparation of this chapter, those problems which bear directly on the theory of solar structure are emphasized.

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Department of Astronomy, University of California, Los Angeles, CA, 90024, USA
Roger K. Ulrich

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Center Space Science and Astrophysics, Standford University, Standford, California, USA
Peter A. Sturrock
High Altitude Observatory, National Center for Atmospheric Research, Boulder, Colorado, USA
Thomas E. Holzer & Dimitri M. Mihalas &
Astronomy Department, University of California, Los Angeles, California, USA
Roger K. Ulrich

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Ulrich, R.K. (1986). Solar Internal Stresses: Rotation and Magnetic Fields. In: Sturrock, P.A., Holzer, T.E., Mihalas, D.M., Ulrich, R.K. (eds) Physics of the Sun. Geophysics and Astrophysics Monographs, vol 24. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-5253-9_6

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DOI: https://doi.org/10.1007/978-94-009-5253-9_6
Publisher Name: Springer, Dordrecht
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